The hunt is on for orbiting pairs of supermassive black holes on the verge of collision. Researchers at Rochester Institute of Technology have built the first simulation that could lead scientists to them.
The predictive model tells astronomers how supermassive black hole
binaries nearing merger at the center of active galaxies would look like
through a modern telescope. The strong gravitational pull drawing the
two supermassive black holes together creates violent shocks in
surrounding gas producing light in the ultraviolet and X-ray
wavelengths. Because current technology is unable to directly observe
the gravitational wave frequency made by supermassive black hole
binaries, scientists observe and measure light emitted along the
electromagnetic spectrum and infer the boundaries of what they can yet
see.
Predicting the characteristic light signals and the timing of their
occurrence will help scientists identify these monster collisions with
existing and future telescopes and better understand what is happening
at the hearts of most galaxies, according to Manuela Campanelli,
director of RIT’s Center for Computational Relativity and Gravitation and a co-author of the new study.
Findings from the paper, “Electromagnetic emission from supermassive binary black holes approaching merger,” appeared in the Oct. 2 issue of The Astrophysical Journal.
The study builds on a prior RIT study
that suggests three gas disks as the light sources: two small companion
disk of accreting gas feed each supermassive black hole; and a larger
disk that contains the scenario playing out within its boundaries.
The computational model applies multi-messenger astronomy by combining
information gathered from light- and gravitational waves, and
high-energy particles. The mini-movies illustrating the simulation are
the first to fully visualize the effects of Einstein’s general theory of
relativity on the light and particles surrounding and passing between
supermassive black holes orbiting each other.
“These are really beautiful images,” said Stéphane d’Ascoli, first
author on the paper and a doctoral student at École Normale Supérieure
in Paris. D’Ascoli collaborated with researchers at RIT’s Center for Computational Relativity and Gravitation, where he was a Visiting Scholar and Graduate Student Intern.
“You can see gravitational lensing and subtle effects we weren’t
expecting, like ‘eyebrows,’ these secondary images of a black hole
created by the way that light passes through the system,” he said.
D’Ascoli worked closely with Campanelli, who had initiated the project nine years ago, and with co-author and former post-doctoral fellow Scott Noble, now at NASA Goddard Space Flight Center. Additional co-authors on the paper include Dennis Bowen and Vassilios Mewes, Ph.D. students at RIT; and Julian Krolik from Johns Hopkins University.
“Identifying the light signatures from supermassive black hole binaries
by some of the many electromagnetic telescopes operating now could
jump-start the field of multimessenger astronomy and sharply refine our
estimates of the population and evolution of supermassive black holes as
well as guiding planning and development of space-based gravitational
wave observatories,” Campanelli said.
Campanelli’s early research was instrumental to the first direct
detection of stellar-mass binary black holes and discovery of
gravitational waves by the LIGO-Virgo Collaboration. Stellar mass black
holes result from supernovae explosions; supermassive black holes form
when galaxies merge and drag along an entourage of gas and dust clouds,
stars and planets.
“We know galaxies with central supermassive black holes combine all the
time in the universe, yet we only see a small fraction of galaxies with
two supermassive black holes near their center,” Noble said. “The ones
we do see are not close enough to be emitting strong gravitational wave
signals because they are too far away from each other. We are after
seeing—with light—the close pairs, what we call binaries, for the first
time.”
Campanelli’s team was one of the first to computationally simulate and
predict gravitational wave signals from a stellar mass black hole merger
a decade before LIGO directly observed the waveforms.
Future observatories like the Laser Interferometer Space Antenna
(LISA), led by the European Space Agency, someday could directly detect
gravitational waves from merging supermassive black holes. Ground-based
observatories are unable to capture the long wavelengths of supermassive
black holes. RIT’s Center for Computational Relativity are members of
the LISA consortium.
The simulation ran on the National Center for Supercomputing
Applications’ Blue Waters supercomputer at the University of Illinois at
Urbana Champaign. Campanelli’s team was recently awarded additional
time on Blue Waters to continue developing their models.
by Susan Gawlowicz
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by Susan Gawlowicz
Follow Susan Gawlowicz on Twitter
Follow RITNEWS on Twitter
Videos available:
Simulation Reveals Spiraling Supermassive Black Holes: Gas
glows brightly in this computer simulation of supermassive black holes
only 40 orbits from merging. Models like this may eventually help
scientists pinpoint real examples of these powerful binary systems.
Credit: NASA’s Goddard Space Flight Center
360-degree Simulated View of the Sky Between Two Supermassive Black Holes:
This 360-degree video places the viewer in the middle of two circling
supermassive black holes around 18.6 million miles (30 million
kilometers) apart with an orbital period of 46 minutes. The simulation
shows how the black holes distort the starry background and capture
light, producing black hole silhouettes. A distinctive feature called a
photon ring outlines the black holes. The entire system would have
around 1 million times the Sun’s mass. Credit: NASA’s Goddard Space
Flight Center; background, ESA/Gaia/DPAC
